Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4060F1.ps} \end{figure}$ Figure 1: The magnitude-redshift diagram for all the galaxies in the spectroscopic sample to $K_{\rm s}<20$ . Filled circles represent galaxies identified spectroscopically, while empty squares are unidentified or unobserved galaxies plotted at $z=z_{\rm phot}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4060F2.ps} \end{figure}$ Figure 2: k-corrections colors (see text) as a function of redshift: $J_{\rm rest}-K_{\rm s}$ (top panel) and $K_{\rm s,rest}-K_{\rm s}$ (bottom panel). Different curves are derived from different spectral models which at low redshift reproduce spectra and colors of local E, S0, Sa, Sb, Sc, Im (solid lines from bottom to top at z>1) and dusty star-forming galaxies (dashed line; see text). Dotted line shows the $2.5 \log (1+z)$ term for comparison.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4060F3.ps} \end{figure}$ Figure 3: The color-redshift ( $R-K_{\rm s}$ vs. z) diagram for galaxies in the spectroscopic sample to $K_{\rm s}<20$ . Different symbols as in Fig. 1. Arrows indicate $3 \sigma$ lower limits in $R-K_{\rm s}$ colors for objects not detected in the R band. The curves show different spectral models as in Fig. 2.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4060F4.ps} \end{figure}$ Figure 4: The absolute J and $K_{\rm s}$ magnitudes as a function of redshift derived (see text) for all galaxies in the spectroscopic sample to $K_{\rm s}<20$ . Symbols as in Fig. 1. Local estimates of M^*_J and $M^*_{K_{\rm s}}$ (dotted horizontal lines) from Cole et al. (2001).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4060F5.ps} \end{figure}$ Figure 5: The rest-frame J-band Luminosity Function in the redshift bins: $z_{\rm mean}\simeq 0.5$ (top panel) $z_{\rm mean}\simeq 1.0$ (middle panel) and $z_{\rm mean}\simeq 1.5$ (bottom panel). Points have been derived from $1/V_{\rm max}$ analysis (open circles using only spectroscopic z and weighted incompleteness corrections, while filled small dots using both spectroscopic and photometric z, see Sect. 4.1), while solid curves are the LF Schechter fits derived from the STY maximum likelihood analysis (thin solid lines are the fits obtained fixing the $\alpha$ parameter at the local value, see text). The dotted curves and vertical dotted lines show the local LF in the J-band and M^*_J at z=0 from Cole et al. (2001).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4060F6.ps} \end{figure}$ Figure 6: The same as in Fig. 5, but for the rest-frame $K_{\rm s}$ -band. The dotted curves and vertical dotted lines show the local LF in the $K_{\rm s}$ -band and M^*_K at z=0 from Cole et al. (2001), while dashed curves show the local LF from Kochanek et al. (2001).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4060F7.ps} \end{figure}$ Figure 7: Rest-frame $K_{\rm s}$ -band Luminosity Function in two redshift bins: $z_{\rm mean}\simeq 0.5$ (top panel) $z_{\rm mean}\simeq 1.0$ (bottom panel). Points and lines derive from $1/V_{\rm max}$ and STY analysis for early (filled symbols and dotted lines) and late (open symbols and dashed lines) galaxies respectively. The solid curves are the STY LF for the total sample in the $K_{\rm s}$ -band as in Fig. 6.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4060F8.ps} \end{figure}$ Figure 8: $R-K_{\rm s}$ colors vs. rest-frame absolute $K_{\rm s}$ magnitudes for K20 galaxy sample in 3 different redshift bins. Circles represent galaxies identified spectroscopically, while squares are unidentified or unobserved galaxies plotted at $z=z_{\rm phot}$ . In each redshift bin empty and filled symbols refer to galaxies with $z<z_{\rm mean}$ and $z\ge z_{\rm mean}$ , respectively.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4060F9.ps} \end{figure}$ Figure 9: Comoving luminosity density in J- (top panel) and $K_{\rm s}$ -bands (bottom panel). The filled circles are the value derived directly from observations (see text), while open circles are the "LF-corrected'' estimates. The solid lines show the best-fit power laws. The open squares are from Cole et al. (2001).
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{H406010a.ps}\hspace*{2mm} \includegraphics[width=8.6cm,clip]{H406010b.ps} \end{figure}$ Figure 10: The rest-frame $K_{\rm s}$ -band Luminosity Function in the redshift bins: $z_{\rm mean}\simeq 0.5$ (top panels) $z_{\rm mean}\simeq 1.0$ (middle panels) and $z_{\rm mean}\simeq 1.5$ (bottom panels) compared to PLE (right panels) and HMM (left panels) models. We have used the models closer to $z_{\rm mean}$ or interpolated between different redshifts. Data points derive from $1/V_{\rm max}$ analysis, while dotted curves are the LF Schechter fit derived from STY analysis. We have corrected the data on average by -0.2 magnitude because photometric selection effects (see text).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4060F11.ps} \end{figure}$ Figure 11: Comoving number density of luminous galaxies ( $M_{K_{\rm s}}<-25.5+5\log~ h_{70}$ ) in the $K_{\rm s}$ -bands. The open circles are the values derived directly from observations, while the filled square is from Cole et al. (2001). The different lines show models as in Fig. 10.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4060F12.ps} \end{figure}$ Figure 12: Left panel: $R-K_{\rm s}$ colors vs. rest-frame absolute $K_{\rm s}$ magnitudes for z=1.05 GIF simulated catalogue (small dots) and data (circles) at 0.75<z<1.3 ( $z_{\rm mean}\simeq 1$ ) (empty and filled circles refer to z<1 and z>1 respectively). Vertical dashed line represents approximately the completeness magnitude limit of GIF catalogue corresponding to its mass limit (see text). Right panel: color distribution of high-luminosity galaxies ( $M_{K_{\rm s}}-5\log ~h_{70}<-24.5$ ) observed (dotted line) and simulated (continue line), normalized to the same comoving volume.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4060F13.ps} \end{figure}$ Figure 13: Predicted SIRTF+IRAC number densities for galaxies with z<2 derived from K20 sample (see text) as a function of AB magnitudes at 3 different wavelengths ( $\lambda=3.6,4.5,5.8~\mu$ m). Histograms refer to $K_{\rm s}<20$ galaxies in our sample in the indicated redshift ranges, while lines have been derived from K20 LFs extended to fainter luminosities (using the flat slope in the highest z range). Vertical dashed lines refer to GOODS flux limits at the different wavelengths.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4060F1.ps} \end{figure}$	Figure 1: The magnitude-redshift diagram for all the galaxies in the spectroscopic sample to $K_{\rm s}<20$ . Filled circles represent galaxies identified spectroscopically, while empty squares are unidentified or unobserved galaxies plotted at $z=z_{\rm phot}$ .
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4060F3.ps} \end{figure}$	Figure 3: The color-redshift ( $R-K_{\rm s}$ vs. z) diagram for galaxies in the spectroscopic sample to $K_{\rm s}<20$ . Different symbols as in Fig. 1. Arrows indicate $3 \sigma$ lower limits in $R-K_{\rm s}$ colors for objects not detected in the R band. The curves show different spectral models as in Fig. 2.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4060F4.ps} \end{figure}$	Figure 4: The absolute J and $K_{\rm s}$ magnitudes as a function of redshift derived (see text) for all galaxies in the spectroscopic sample to $K_{\rm s}<20$ . Symbols as in Fig. 1. Local estimates of M^_J and $M^_{K_{\rm s}}$ (dotted horizontal lines) from Cole et al. (2001).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4060F6.ps} \end{figure}$	Figure 6: The same as in Fig. 5, but for the rest-frame $K_{\rm s}$ -band. The dotted curves and vertical dotted lines show the local LF in the $K_{\rm s}$ -band and M^*_K at z=0 from Cole et al. (2001), while dashed curves show the local LF from Kochanek et al. (2001).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4060F9.ps} \end{figure}$	Figure 9: Comoving luminosity density in J- (top panel) and $K_{\rm s}$ -bands (bottom panel). The filled circles are the value derived directly from observations (see text), while open circles are the "LF-corrected'' estimates. The solid lines show the best-fit power laws. The open squares are from Cole et al. (2001).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4060F11.ps} \end{figure}$	Figure 11: Comoving number density of luminous galaxies ( $M_{K_{\rm s}}<-25.5+5\log~ h_{70}$ ) in the $K_{\rm s}$ -bands. The open circles are the values derived directly from observations, while the filled square is from Cole et al. (2001). The different lines show models as in Fig. 10.
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